2006/06/22 by Joshua D. Simon, Francisco Prada, J. M. Vı́lchez +3 · 1 citation
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Dwarf galaxy #Elliptical galaxy #Fundamental plane (elliptical galaxies) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy rotation curve #Geometry #Interacting galaxy #Irregular galaxy #Lenticular galaxy #Line (geometry) #Local Group #Metallicity #Physics #Stellar, planetary, and galactic studies #Supernova #Surface brightness #Surface brightness fluctuation #astro-ph
paper · pdf · doi:10.1086/507117
published as Astrophys.J.649:709-721,2006 · 14 pages, 14 figures (5 in color). Accepted for publication in ApJ
arxiv created 2006/06/22 · openalex publication_date 2006/09/27 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We show that there are strong local correlations between metallicity, surface brightness, and dynamical mass-to-light ratio with M33, analogous to the fundamental line of dwarf galaxies identified by Prada & Burkert. Using near-infrared imaging from 2MASS, the published rotation curve of M33, and literature measurements of the metallicities of H II regions and supergiant stars, we demonstrate that these correlations hold for points at radial distances between 140 pc and 6.2 kpc from the center of the galaxy. At a given metallicity or surface brightness, M33 has a mass-to-light ratio approximately 4 times as large as the Local Group dwarf galaxies; other than this constant offset, we see broad agreement between the M33 and dwarf galaxy data. We use analytical arguments to show that at least two of the three fundamental line correlations are basic properties of disk galaxies that can be derived from very general assumptions. We investigate the effect of supernova feedback on the fundamental line with numerical models and conclude that while feedback clearly controls the scatter in the fundamental line, it is not needed to create the fundamental line itself, in agreement with our analytical calculations. We also compare the M33 data with measurements of a simulated disk galaxy, finding that the simulation reproduces the trends in the data correctly and matches the fundamental line, although the metallicity of the simulated galaxy is too high, and the surface brightness is lower than that of M33.